Issue 
A&A
Volume 547, November 2012



Article Number  A64  
Number of page(s)  11  
Section  Astrophysical processes  
DOI  https://doi.org/10.1051/00046361/201118511  
Published online  29 October 2012 
Angular momentum transport and turbulence in laboratory models of Keplerian flows
^{1}
Department of Physics and Center for Nonlinear DynamicsUniversity of
Texas,
Austin,
TX,
78712,
USA
email: mpaolett@gmail.com
^{2}
Physics of Fluids Group, Faculty of Science and Technology, Mesa+
Institute and Burgers Center for Fluid Dynamics, University of Twente,
7500AE
Enschede, The
Netherlands
^{3}
CNRS URA 2464 SPHYNX/SPEC/IRAMIS/DSM, CEA Saclay,
91191
GifsurYvette,
France
^{4}
Departments of Physics and Geology, Institute for Research in
Electronics and Applied Physics, Institute for Physical Science and Technology,
University of Maryland, College
Park, MD
20742,
USA
email: lathrop@umd.edu
Received:
23
November
2011
Accepted:
5
September
2012
We present angular momentum transport (torque) measurements in two recent experimental studies of the turbulent flow between independently rotating cylinders. In addition to these studies, we reanalyze prior torque measurements to expand the range of control parameters for the experimental TaylorCouette flows. We find that the torque may be described as a product of functions that depend only on the Reynolds number, which describes the turbulent driving intensity, and the rotation number, which characterizes the effects of global rotation. For a given Reynolds number, the global angular momentum transport for Keplerianlike flow profiles is approximately 14% of the maximum achievable transport rate. We estimate that this level of transport would produce an accretion rate of Ṁ/Ṁ_{0}~10^{3} in astrophysical disks. We argue that this level of transport from hydrodynamics alone could be significant. We also discuss the possible role of finitesize effects in triggering or sustaining turbulence in our laboratory experiments.
Key words: accretion, accretion disks / turbulence / methods: laboratory / hydrodynamics
© ESO, 2012
1. Introduction
Astrophysical disks are ubiquitous in the universe, orbiting around a wide panel of massive objects, from black holes to stars. An essential ingredient of their dynamics is the radial transport of angular momentum that governs the rate of material falling onto the central object. Realistic models of this process are impeded by the complexity of the disk dynamics, including a wide variety of processes such as general relativistic effects, selfgravitation, radiation, dynamics of plasma magnetic fields and turbulence. In particular, the contribution from hydrodynamics to the angular momentum transport in such astrophysical flows is not yet understood.
A natural firststep in the construction of a robust model is to consider the minimal list of ingredients that can capture and reproduce the observed disk properties. Such a model has been proposed several decades ago by Shakura & Sunyaev (1973) and Pringle (1981), and was given the name α disks. In that model, the radial transport of angular momentum is parameterized by a turbulent viscosity coefficient that needs to be prescribed or measured. In the past, there have been several attempts to estimate this coefficient from an analytical closure model (Dubrulle 1992), numerical simulations (see e.g. Rozyczka & Spruit 1993; Brandenburg et al. 1995; Abramowicz et al. 1996; Stone et al. 1996; Drecker et al. 1998; Beckwith et al. 2011; and a recent review by King et al. 2007, and references therein), or using theoretical arguments (Canuto et al. 1984; Mukhopadhyay 2008).
An alternative promising option, as recognized by Zeldovich (1981) and Richard & Zahn (1999), is offered by instead focusing on laboratory experiments. Indeed, it may be shown (Hersant et al. 2005) that under simple but well founded approximations the equations governing an α disk are similar to the equation of motion of an incompressible rotating shear flow, with penetrable boundary conditions and cylindrical geometry. This can be modeled in the TaylorCouette flow (see Fig. 1), a fluid layer sheared between two independently rotating, coaxial cylinders.
These proposals motivated several studies of the transport properties in rotating shear flows, with contradicting conclusions. From the numerical point of view, the problem has been mainly tackled in the astrophysical community using the socalled shearing sheet approximation either without explicit viscosity (Balbus et al. 1996; Hawley et al. 1999), or with explicit viscosity (Lesur & Longaretti 2005) at resolutions ranging from 32^{3} to 256^{3}. This method is often seen as the simplest way to deal with the (unknown) disk boundary conditions, but it has some limitations as discussed in past work (Pumir 1996; Umurhan & Regev 2004; Fromang & Papaloizou 2007). While Balbus et al. (1996); Hawley et al. (1999) did not use explicit viscosity, thereby making it difficult to directly define a Reynolds number, they estimated that their simulations achieved Re ~ 10^{3}−10^{4}. In their case, they did not find any evidence for a subcritical transition to turbulence for Keplerian flows, which they determined to be completely stabilized by the Coriolis force. The simulations of Lesur & Longaretti (2005) at N^{3} = 128^{3} could achieve Re ≈ 4 × 10^{4}, according to their estimation. They concluded, on the other hand, that Keplerian like flows could exhibit turbulence, although the turbulence intensity may be too weak to account for the rate of energy dissipation observed. This has motivated us to experimentally explore Reynolds number up to Re = 4 × 10^{6}, a value that is beyond present computational efforts.
The overwhelming computational requirements needed to obtain larger Reynolds numbers motivate an alternate approach to explore the transport properties of TaylorCouette flow through laboratory experiments, which can obtain much larger Reynolds numbers, as we present here. Depending upon the community, the strength of the turbulent transport is quantified in various ways. The most basic quantification (Wendt 1933) is the one through the torque T which is necessary to keep the inner cylinder rotating at a given velocity. The dimensionless version thereof is G = T/(L_{mid}ρν^{2}), where ρ is the fluid density, ν its kinematic viscosity and L_{mid} the effective length of the cylinders (Paoletti & Lathrop 2011). Eckhardt et al. (2007b) and van Gils et al. (2011b) used Nu_{ω} = G/G_{lam}, where G_{lam} is the laminar torque, to quantify the angular velocity flux from the inner to the outer cylinder, in order to highlight the analogy between TaylorCouette and RayleighBénard flow (Dubrulle & Hersant 2002; Eckhardt et al. 2007b,a). The engineering community prefers the dragcoefficient c_{f} = G/Re^{2}, where and η = a/b is the radius ratio and Re_{1/2} the Reynolds number of the inner/outer cylinder. In the astrophysics community, the same information is often expressed in terms of the β coefficient, defined by β = 2Gη^{2}/(π(1 − η)^{4}Re^{2}) = 2η^{2}c_{f}/(π(1 − η)^{4}), which can be interpreted as a dimensionless turbulent viscosity.
By reexamining previous data obtained by Wendt (1933) and Taylor (1936), Richard & Zahn (1999) showed that the βparameter is on the order of β_{RZ} ~ 10^{5} for Keplerian disks. A more complete analysis, including results of new experiments on a classical TaylorCouette flow from Richard (2001), led to the same conclusion (Dubrulle et al. 2005). In contrast, an original experiment, built in Princeton (Ji et al. 2006) so as to minimize end effects, measured a β coefficient through radial Reynolds stresses and obtained a value smaller by more than an order of magnitude β_{P} ~ 7 × 10^{7}. Furthermore, the Princeton experiments could not distinguish the angular momentum transport in Keplerian flows from their measurements in solidbody rotation, where the cylinders rotate together thereby resulting in zero angular momentum transport.
Fig. 1 TaylorCouette flow may be used to study angular momentum transport in rotating shear flows. The fluid is sheared between two independently rotating cylinders of radii a < b that rotate at angular velocities Ω_{1} and Ω_{2} for the inner and outer cylinders, respectively. Although the total fluid height is given by L, some experiments only measure the contribution to the torque over a central section of length L_{mid} to minimize end effects, as in (Lathrop et al. 1992b,a; Lewis & Swinney 1999; van den Berg et al. 2003, 2005, 2007; Paoletti & Lathrop 2011; van Gils et al. 2011b). 
In the present contribution, we report precise global angular momentum transport (torque) measurements in two independent experiments performed at very large Reynolds number and compute the resulting β coefficient for different rotation profiles. To further study the scaling of angular momentum transport in rotating shear flows, we compare our measurements to those of Wendt (1933), Taylor (1936) and Richard (2001), Dubrulle et al. (2005). We find a universal scaling of the torque for various rotation profiles that captures the effects of the various geometries used in the experiments summarized here.
2. Apparatus and experimental details
2.1. Apparatus: generalities
The experiments presented here all examine the transport of angular momentum (torque) in classical TaylorCouette flow. Figure 1 shows a schematic representation of our experiments. The fluid is contained between concentric cylinders of radii a < b. The inner (outer) cylinder rotates at an angular velocity of Ω_{1}(Ω_{2}). The overall height of the fluid contained between the axial boundaries is given by the length L. The geometry of a particular TaylorCouette flow apparatus is often defined in dimensionless form by the radius ratio η ≡ a/b and the aspect ratio Γ ≡ L/(b − a).
The ideal Couette flow is infinite in axial extent. As such, several methods have been employed to handle the finitesize effects that are present in any laboratory experiment. The most common case has the axial boundaries rotate with one of the two cylinders. In other experiments, the axial boundaries are divided at the midgap and have the inner (outer) portion rotate with the inner (outer) cylinder. This splitring approach has been further developed to allow for pairs of rings that can independently rotate with respect to the cylinders. Allowing the axial boundaries to independently rotate aids in the suppression of finitesize effects (Ji et al. 2006; Schartman et al. 2009; Burin et al. 2010).
Parameters used in the experiments discussed here.
The data that we analyze and present stems from several different experiments, which are summarized in Table 1. The early experiments by Wendt (1933) measured the torque required to drive the inner cylinder for three values of η. The system had a free surface at the top, although we quote an effective aspect ratio defined using the axial length of the apparatus. The data from Taylor (1936) determined the scaling of the torque for several values of η with the inner cylinder stationary (Ω_{1} = 0). Richard’s experiments (Richard 2001; Dubrulle et al. 2005) did not directly measure the torque. Instead, critical Reynolds numbers for various transitions were observed and the analysis presented by Dubrulle et al. (2005) was used to estimate the corresponding torque. We do not present data from the experiments of Ji et al. (2006), but rather use their reported measurements as a basis for comparison, as detailed in Sect. 4. The two most recent experiments by Paoletti & Lathrop (2011) and van Gils et al. (2011b) are further described in the forthcoming sections.
2.2. Apparatus: the Maryland experiment
The experiments presented by Paoletti & Lathrop (2011), henceforth referred to as the Maryland experiment, are conducted in the apparatus constructed by Lathrop et al. (1992b,a), which was modified to allow the outer cylinder to rotate independently. The outer cylinder is an anodized aluminum cylinder with the same physical dimensions as in Lathrop et al. (1992b,a); Lewis & Swinney (1999), specifically b = 22.085 cm and a working fluid height L = 69.50 cm. The inner cylinder is stainless steel with a radius a = 16.000 cm yielding a radius ratio η = 0.7245 and an aspect ratio Γ = 11.47. The inner cylinder is rotated up to Ω_{1}/2π = 20 s^{1} while the outer cylinder may be rotated in either direction up to Ω_{2}/2π = 10 s^{1}. Both angular velocities are measured by shaft encoders and controlled to within 0.2% of the set value.
The axial boundaries in the Maryland experiment rotate with the outer cylinder. To reduce end effects in the torque measurements the inner cylinder is divided axially into three sections of length 15.69, 40.64 and 15.69 cm (see schematics in Lathrop et al. 1992b,a). Only the central section of length L_{mid} = 40.64 cm (see Fig. 1) senses the torque of the fluid as described in Lathrop et al. (1992b,a). The regions of the flow within 2.58 gap widths from each of the axial boundaries, where secondary circulation setup by finite boundaries is strongest, are avoided in the torque measurements.
TaylorCouette control parameters related to some astrophysical disks, as computed by Hersant et al. (2005).
The desired accuracy of our measurements requires that the temperature of the water be precisely controlled. In contrast to prior experiments (Lathrop et al. 1992b,a; Lewis & Swinney 1999; van den Berg et al. 2003, 2005, 2007; van Gils et al. 2011b) where the system was cooled at the axial boundaries, we control the temperature of the water by heating and cooling the outer cylinder. This allows the working fluid to be temperaturecontrolled along the entire axial length of the experiment, yielding a 6.5 fold increase in the temperaturecontrolled surface area. This is particularly important for Rayleighstable flows, where mixing is greatly reduced. In our experiments the temperature is 50 ± 0.02 °C yielding a kinematic fluid viscosity of ν = 5.5 × 10^{3} cm^{2}/s, except for Re > 2 × 10^{6} where T = 90 °C and ν = 3.2 × 10^{3} cm^{2}/s.
2.3. Apparatus: the Twente experiment
The Twente turbulent TaylorCouette (called T^{3}C) facility, here referred to as the Twente experiment, is described in great detail in van Gils et al. (2011a). In short, the working fluid height is L = 92.7 cm, has an inner radius of a = 20.0 cm and an outer radius of b = 27.94 cm. The maximum inner and outer angular velocities are Ω_{1}/2π = 20 Hz and Ω_{2}/2π = 10 Hz, respectively. The system is fully temperature controlled through cooling of the upper and lower end plates, which corotate with the outer cylinder. The system is operated with water at a temperature of 20 °C, resulting in a kinematic viscosity of ν = 1.04 × 10^{2} cm^{2}/s. The torque is measured over the middle part of the inner cylinder of height L_{mid} = 53.6 cm to minimize the influence of the endplates (similar to Lathrop et al. 1992b,a). The torque is measured by a load cell imbedded inside the middle section of the inner cylinder in both the Twente and Maryland experiments, in contrast to measuring the torque on the drive shaft that would be affected by mechanical seals in the end plates or by velocimetry measurements, as in the Princeton experiments (Ji et al. 2006; Schartman et al. 2009; Burin et al. 2010; Schartman et al. 2012).
2.4. Control parameters
The analysis of our results is simplified by a proper choice of the control parameters. As in Dubrulle et al. (2005), we use the following three dimensionless control parameters, which fully describe the geometry and specify the state of the dynamical TaylorCouette system: where Re_{1} = aΩ_{1}d/ν and Re_{2} = bΩ_{2}d/ν are the Reynolds number of the inner and outer cylinder and d = (b − a) is the gap width.
The above control parameters have been introduced so that their definitions apply to rotating shear flows in general and not strictly only to the TaylorCouette geometry. It is very easy in this formulation to relate the TaylorCouette flow to the shearing sheet (plane Couette flow with rotation), by considering the limit R_{C} → 0. The linear stability properties of the fluid can also be neatly recast using these control parameters. In the inviscid limit (Re → ∞), and for axisymmetric disturbances, the linear stability properties of the flow are governed by the Rayleigh criterion, namely that the fluid is stable if the Rayleigh discriminant is everywhere positive: (4)where L(r) = r^{2}Ω(r) is the specific angular momentum. Applying this criterion to the laminar profile leads to (5)Since ab/r^{2} varies between 1/η and η, one obtains that in the inviscid limit, the flow is unstable against infinitesimal axisymmetric disturbances when , where , respectively , are the marginal stability thresholds in the inviscid limit (superscript ∞) in the cyclonic case (R_{Ω} > 0, subscript + ), and anticyclonic case (R_{Ω} < 0, subscript −). This means that, in the anticyclonic case, any flow such that R_{Ω} < −1 is linearly stable against axisymmetric disturbances. However, it may be nonlinearly stable or unstable against nonaxisymmetric disturbances, as found in the experiments described here.
In the present paper, we determine the intensity of the momentum transport by measuring the torque required to drive the inner cylinder for a given set of parameters (Re,R_{Ω}). Measurements described here suggest that at large enough Reynolds number, the nondimensional torque G = T/(ρν^{2}L_{mid}), where T is the torque, ρ the fluid density, ν the kinematic viscosity and L_{mid} is defined in Fig. 1, varies approximately as G ~ Re^{α} with 1.75 < α(Re) < 1.85, even for Rayleighstable flows. While this scaling exceeds the laminar case (G ~ Re), we note that these exponents are less than a simple dimensional argument would give: Such an argument would say that in a fully turbulent regime the transport properties could not depend on the molecular viscosity, which would imply that the quantity c_{f} ~ G/Re^{2} is Reynolds number independent. The deviations from G ~ Re^{2} mean that the viscosity is always relevant for the transport, due to its dominance in the boundary layers. Only when the boundary layers are sufficiently disturbed by introducing wall roughness does one obtain G ~ Re^{2}, as we have shown in our previous work (van den Berg et al. 2003).
2.5. Astrophysically relevant quantity
In the astrophysical context, one often considers asymptotic angular velocity profiles of the form Ω(r) ~ r^{−q} where q characterizes the flow. In that case q = −∂lnΩ/∂lnr = −2/R_{Ω}, which relates astrophysical profiles in the control parameters space of TaylorCouette flows. For Keplerian flow, q = 3/2 resulting in R_{Ω} = −4/3, which is an example of a linearly stable, anticyclonic flow. While Keplerian profiles cannot be precisely achieved by TaylorCouette flows, states with R_{Ω} < −1 are all linearly stable, anticyclonic flows that may be used to approximate astrophysical settings. We will refer to cases with R_{Ω} < −1 as quasiKeplerian, as in Ji et al. (2006).
Astrophysical disks are very wide with a ≪ b. Therefore, their geometrical global value of R_{C} → ∞. In a local description of disks, one often considers the shearing sheet approximation, in which η → 1, so that R_{C} → 0, as in planeCouette flow. Here, we focus on global properties and consider only the limit η → 0 applicable to disks in the discussion. As a result of their astronomical size, the Reynolds numbers associated with accretion disks are very large. To give a few specific examples, parameters for typical T Tauri and Fu Ori stars have been computed by Hersant et al. (2005) and are given in Table 2.
In disks, angular momentum transport intensity is quantified through the accretion rate Ṁ. In fact, as was shown in (Dubrulle et al. 2005; Hersant et al. 2005), this rate is directly related to the turbulent viscosity and the dimensionless torque. This concept may be understood in the following way: pressure gradients substantially balance centrifugal forces that develop in (incompressible) laboratory flows. Keplerian disks, however, balance the centrifugal force with gravitational attraction. Thus when angular momentum is transported radially outward, accretion disk matter responds by falling radially inward at the rate Ṁ. The flux of angular momentum, which is proportional to G, is thereby related to the accretion rate Ṁ by (Dubrulle et al. 2005; Hersant et al. 2005), (6)where β is a turbulent viscosity parameter such that ν_{t} = βSr^{2}, with S a velocity shear, and Ṁ_{0} is an effective accretion rate given by the mean surface density , the disk inner radius a, mean radius ,the mean angular velocity and the mean disk height through (7)As such, measurements of G/Re^{2} in laboratory experiments may be used to estimate the hydrodynamical contribution to angular momentum transport in accretion disks.
Fig. 2 a) Our experiments span a large range of the Reynolds number Re, which controls the turbulence intensity, and the rotation number R_{Ω}, introduced by Dubrulle et al. (2005), which compares shear to overall rotation. The rotation number can be used to distinguish between Rayleighstable flows (R_{Ω} ≤ −1 or R_{Ω} ≥ (1 − η)/η) and those that are linearly unstable (−1 < R_{Ω} < (1 − η)/η). b) All of our measurements for −1 < R_{Ω} < 0.38 are well above the linear stability curve (blue line) described by Esser & Grossmann (1996) and given by Eq. (8). The data are taken from separate experiments by van Gils et al. (2011b) (red squares) and (Paoletti & Lathrop 2011) (black circles). 
Fig. 3 The scaling of the dimensionless torque G with the Reynolds number Re is independent of the rotation number R_{Ω}, however the amplitude varies as in Paoletti & Lathrop (2011); van Gils et al. (2011b). The measurements by Paoletti & Lathrop (2011) are in black circles while the data from van Gils et al. (2011b) are shown by red squares. The thick blue line indicates the theoretical value for purely laminar flow, where angular momentum is transported only by molecular viscosity. 
3. Results
We study the scaling of the dimensionless torque G over a range of Reynolds numbers for various constant rotation numbers (see Fig. 2), spanning a wide variety of flow states, including linearly stable cyclonic and anticyclonic flows as well as linearly unstable states. Esser & Grossmann (1996) derived an analytical expression that approximates the boundary for linear stability for all radius ratios and cylinder rotation rate ratios. Their result for the critical Reynolds number Re_{c} may be expressed using the above control parameters, as in Eqs. (16) and (17) in Dubrulle et al. (2005): (8)with where Δ(x) is a function equal to x if x < 1 and equal to 1 if x > 1. Equation (8) may be used to determine the stability boundary for the experiments described in Table 1. As shown in Fig. 2b, all of our measurements for −1 < R_{Ω} < 0.38 are orders of magnitude above the laminar stability boundary. For R_{Ω} < −1 or R_{Ω} > 0.38 the system is linearly stable for our radius ratios, although it may be possible for the system to undergo a subcritical transition to turbulence. Corresponding torque measurements from the Twente experiment are shown as red squares in Fig. 3 while the data from Maryland are represented by black circles.
3.1. Existence of turbulence
In laminar flow, angular momentum is transported only by molecular viscosity, so that the dimensionless torque G is proportional to Re, with the prefactor depending upon R_{Ω}. In Fig. 3, we show the expected laminar angular momentum transport (blue line) for the range of Re explored in this study for the case Ω_{2} = 0. As can be seen all the torque measurements considered differ from the theoretical expectation for laminar flow in two ways: (i) they increase faster than Re and (ii) they are much higher than the theoretical laminar value. This is an indication that the fluid is turbulent, with enhanced angular momentum transport in all the cases reported here. Note that these cases encompass several situations with R_{Ω} < −1 (linearly stable anticyclonic flow) and R_{Ω} > 0.4 (linearly stable cyclonic flow) in addition to many unstable states.
In particular, (approximate) Keplerian flows at R_{Ω} = −4/3 are turbulent at Re ~ 10^{5} in our experiments. This is in agreement with direct, visual observations of Richard (2001), performed at somewhat lower Reynolds number. We argue that this indicates that quasiKeplerian flows can efficiently transport angular momentum in spite of their linear stability. However, the nature of this nonlinear instability remains unclear. We suggest that systematically perturbing quasiKeplerian flow states at lower values of Re while measuring the torque, as in the experiments by Taylor (1936), could aid in the description of this likely nonlinear instability.
3.2. Enhancement of momentum transport
We now try to quantify the enhancement of angular momentum transport with respect to its laminar value, as a function of both Re and R_{Ω}. As in Paoletti & Lathrop (2011); van Gils et al. (2011b), the torque at a given Re may be either increased or reduced depending upon R_{Ω}; the Reynolds number alone is insufficient to describe the transport.
3.2.1. Variation with R_{Ω}
Paoletti & Lathrop (2011) observed that variation of the torque at a given Re shows a pronounced maximum as a function of R_{Ω}. An analogous dependence of the amplitude of an effective powerlaw scaling was also observed by van Gils et al. (2011b). To determine the effects of global rotation, we normalize G for each Re by G(Re,R_{Ω} = 0) (Dubrulle et al. 2005), which we denote as G_{0}. This normalization is different from Fig. 16 in Dubrulle et al. (2005) where G is normalized by G_{∞} ≡ G(Re,Ω_{2} = 0). The dependence of G/G_{0} on R_{Ω} is shown in Fig. 5 with the data from Maryland shown as black circles and Twente in red squares.
Fig. 4 a) The dimensionless torque G normalized by G_{0} ≡ G(Re,R_{Ω} = 0) for different values of the radius ratio η nicely collapses when plotted as function of R_{Ω}. The data from Wendt (1933) are shown as cyan (η = 0.68), blue (η = 0.85) and green (η = 0.935) triangles. Additional radius ratios are examined using the data from Taylor (1936), shown as orange diamonds, Richard (Richard 2001; Dubrulle et al. 2005), given by magenta squares, Paoletti & Lathrop (2011) indicated by black circles and van Gils et al. (2011b) by red circles. The solid lines are fits given by Eq. (12). Keplerian flow states are indicated by the dashed line at R_{Ω} = −4/3. In b) we focus on the peak of the curve shown in a), but only present the data from Twente (van Gils et al. 2011b) (red) and Maryland (Paoletti & Lathrop 2011) (black). The solid line is the fit (12). 
Fig. 5 The dimensionless torque G may be compensated by the fit f(R_{Ω}) given by Eq. (12). The data from both Paoletti & Lathrop (2011) (black circles) and van Gils et al. (2011b) (red squares) agree with the best fit from Lewis & Swinney (1999) for the case where the outer cylinder was stationary (blue line). 
The agreement between the Twente and Maryland measurements is an important check, but not surprising given that the experiments have very similar geometries, measurement techniques and control parameters (see Table 1). Therefore, it remains unclear if the scaling of the normalized torque with R_{Ω} is universal or if it depends upon other parameters, such as the radius ratio η. While the Twente experiment is capable of examining other values of η in future measurements, we may compare our results to previous experiments by Wendt (1933), Taylor (1936) and Richard (2001), which were analyzed by Dubrulle et al. (2005). The parameters of these past experiments are also summarized in Table 1. The measurements of Wendt (triangles), Taylor (orange diamonds) and Richard (magenta squares) are also shown in Fig. 4a.
As can be seen in Fig. 4, the dependence of the normalized torque G/G_{0} on R_{Ω} for various radius ratios in the range 0.68 ≤ η ≤ 0.973 collapse well. The data appear to follow distinct approximate scalings given by (12)Given the rather different span of Re in each experiment and the varying measurement techniques, it is not surprising that a few outliers remain. For example, the values of G/G_{0} from Richard’s experiments (Richard 2001) (magenta squares) were computed using theoretical predictions regarding the correlation between the torque and critical numbers for stability, as described in Dubrulle et al. (2005). The data from Wendt (1933), Taylor (1936), Paoletti & Lathrop (2011) and van Gils et al. (2011b) are direct measurements of the torque, albeit with different apparati and measurement techniques.
3.2.2. Variation with Reynolds number
The fits given in Eq. (12) may be used to compensate the torque to account for the effects of global rotation. Figure 5 shows the dimensionless torque G compensated by the fit f(R_{Ω}) given in Eq. (12) as a function of Re. The data from Twente are shown as red squares while those of Maryland are given by black circles. In both cases, the data agree well with the best fit given by Lewis & Swinney (1999) for the case Ω_{2} = 0 (blue line). This indicates that the amplitude of the torque is affected by global rotation, as measured by G/G_{0}, while the scaling with Re seems to be independent of R_{Ω} in the regime of our investigation. Therefore the torque may be approximately factorized and written as (13)where f(R_{Ω}) is measured in Fig. 4 and fit by Eq. (12) and our measurements of g(Re), shown in Fig. 5, agree with previous measurements, and may be fit by effective powerlaws or logarithmically varying functions such as the Prandtlvon Kármán form (Lathrop et al. 1992b,a; Lewis & Swinney 1999).
3.2.3. Comments
In addition to the observed data collapse, other interesting features arise in the normalized torque scaling with R_{Ω}. The data from Taylor’s experiments (Taylor 1936) were obtained with a stationary inner cylinder (Ω_{1} = 0), and the flow is therefore Rayleighstable. However, the data from Wendt (1933), Maryland (Paoletti & Lathrop 2011) and Twente (van Gils et al. 2011b) over the same range of the rotation number, namely 0 < R_{Ω} < 0.27, are obtained with counterrotating cylinders. This configuration is linearly unstable, yet the measured values of G/G_{0} agree between all four experiments. We argue, as done by Taylor (1936), that the flow states in Taylor’s experiments could not have been laminar and must have undergone a subcritical transition to turbulence.
Paoletti & Lathrop (2011) observed that the torque scaling varied linearly with R_{Ω} in four regions of the parameter space corresponding to: region I: R_{Ω} ≤ −1, region II: −1 < R_{Ω} ≤ −0.10, region III: −0.10 < R_{Ω} < 0.38 and region IV: 0.38 < R_{Ω}, where we have reordered the region numbers to correspond to increasing R_{Ω}. Figure 4 shows that all of the data described here follow the region I–region II and region II–region III crossovers. The crossover between regions I and II corresponds to the Rayleigh stability criterion for all values of η. The crossover between regions II and III occurs at the observed maximum in the normalized torque G/G_{0} as a function of R_{Ω}. While this maximum occurs for all of the Wendt (1933), Maryland (Paoletti & Lathrop 2011) and Twente (van Gils et al. 2011b) datasets, there is no general theoretical prediction for the exact location of this maximum yet.
The last crossover observed by Paoletti and Lathrop, between regions III and IV, corresponded to Ω_{1} = 0 with Ω_{1} > 0 and Ω_{2} < 0 in region III (counterrotation) to Ω_{1} > 0 and Ω_{2} > 0 in region IV (corotation). It is unclear whether this crossover is set by R_{Ω} = 0.38 or whether it always occurs at R_{Ω}(Ω_{1} = 0). The data from Taylor (1936) has Ω_{1} = 0 but given the values of η used in those experiments R_{Ω} < 0.38. The Richard data for R_{Ω} > 0.38 fall below the observations by Maryland, although the scaling with R_{Ω} is similar. It is unclear if this disparity is a result of the analysis used to deduce the torques from Richard’s measurements or the difference in the control parameters from the Maryland experiment (see Table 1). It would be fruitful to have independent, direct measurements of the torque in region IV to compare against those of Maryland at different radius ratios to better understand this final crossover.
Fig. 6 The scaling of a) G/Re^{2}, which is proportional to the accretion rate Ṁ and viscosity parameter β, decays slowly with Re while having an amplitude that varies with the rotation number R_{Ω} (see Fig. 4). b) The effects of global rotation can be accounted for by compensating G/Re^{2} by the fits f(R_{Ω}) given in Eq. (12). The measurements from Twente are shown as red squares. The Maryland data are given by black circles, except for quasiKeplerian flows (R_{Ω} ≤ −1), which are indicated by blue diamonds. The green continuous line is the theoretical fit given in Eq. (14) normalized by f(R_{Ω} = −0.2755), which corresponds to Ω_{2} = 0. 
The Richard and Maryland data both indicate that the observed torque for quasiKeplerian flows states (R_{Ω} ≤ −1) is approximately 14% of the maximum observed torque for a given Reynolds number. This is in contrast to the results of Ji et al. (2006), who deduced that such flow states are “essentially steady” and unable to transport angular momentum hydrodynamically. In addition to the different geometries between the experiments in Ji et al. (2006) and those of Richard and Maryland (see Table 1), the measurement techniques and finitesize effects were different between the experiments. This contrast is further discussed in Sect. 4. Clearly, additional independent measurements of the angular momentum flux for quasiKeplerian flows could aid this debate, as recently discussed by Balbus (2011).
3.2.4. Astrophysical implications
As described in Sect. 2.5, the scaling of the torque with Reynolds number may be used to determine either the turbulent viscosity parameter β or the accretion rate Ṁ through Eq. (6). Our measurements of G/Re^{2}, which is proportional to both β and Ṁ, are shown in Fig. 6a. The measurements from Twente are shown as red squares while those of Maryland are given by black circles. The data indicated by blue diamonds are quasiKeplerian flow states (R_{Ω} ≤ −1) from the Maryland experiment. The quantity G/Re^{2} decreases slowly with Re (only logarithmically, see Dubrulle et al. 2005; Hersant et al. 2005; Grossmann & Lohse 2011) as expected since G ∝ Re^{α} with 1.8 < α(Re) ≤ 2.0 for 10^{5} < Re < ∞ (Lathrop et al. 1992b,a; Lewis & Swinney 1999). The amplitude of G/Re^{2} for a given Re is determined by R_{Ω}. The effects of global rotation may be accounted for by compensating the measurements of G/Re^{2} by f(R_{Ω}) (see. Eq. (12)), as shown in Fig. 6b. As discussed in Dubrulle & Hersant (2002), the scaling may be fit by a logarithmically decaying function, such as: (14)with the values chosen to be K_{7} = 0.4664 and K_{8} = 10^{4} to describe the best fit for the torque scaling provided by Lewis & Swinney (1999) for the case Ω_{2} = 0. An alternative logarithmic dependence between G/Re^{2} and Re has been suggested by Grossmann & Lohse (2011) (for the analogous case of ultimate RayleighBénard flow), and it equally well fits the data.
The expected accretion rate, measured by G/Re^{2} = 3.3 × 10^{3}, for quasiKeplerian flows (blue diamonds in Fig. 6) is approximately 14% of the maximum accretion rate, which occurs for R_{Ω} = −0.10. This corresponds to a value of β_{Md} = 2 × 10^{5} or Ṁ/Ṁ_{0} = 3.3 × 10^{3} at Re = 7 × 10^{5}. Extrapolating towards astrophysical Reynolds numbers by using the formula of Hersant et al. (2005, see Eq. (6)), we get a value of Ṁ/Ṁ_{0} = 10^{3} that is consistent with values observed in disks around T Tauri stars.
4. Discussion
The measured accretion rate for all of our quasiKeplerian flows (R_{Ω} ≤ −1) is approximately 14% of the maximum accretion rate, which occurs at R_{Ω} = −0.10, resulting in β_{Md} = 2 × 10^{5}. This is close to the value computed by Richard and Zahn β_{RZ} = 10^{5} and to the value of Dubrulle et al. (2005)β_{D} = 8 × 10^{6}. This is somewhat surprising given that quasiKeplerian flow profiles are linearly stable while the maximum accretion rate occurs when the cylinders counterrotate, which produces destabilizing shear that dominates the dynamics. This result is in stark contrast to the results presented by Ji et al. (2006) and Schartman et al. (2012), where β_{P} was measured to be an order of magnitude smaller, specifically β_{P} = 7 × 10^{7}. Thus, they concluded that hydrodynamics alone cannot efficiently transport angular momentum in quasiKeplerian flows.
Schartman et al. (2012) state that these incompatible results are caused by differing interpretations of finitesize effects, namely Ekman circulation produced by the axial boundaries. In the Princeton experiments (Ji et al. 2006; Schartman et al. 2009; Burin et al. 2010; Schartman et al. 2012) the aspect ratio is small (Γ ≈ 2) and therefore finitesize effects would likely dominate. To minimize Ekman circulation, their axial boundaries are split into pairs of rings that can independently rotate with respect to the cylinders. This method has been shown to reduce the effects of Ekman circulation in the bulk of the fluid (Schartman et al. 2009). Furthermore, when Ekman circulation is not minimized their measured values of β for quasiKeplerian flows are approximately half of the typical values presented here. Thus, Schartman et al. (2012) argue that our larger values of β are the result of Ekman circulation that is present in other experiments, but is minimized in their apparatus.
We argue, on the other hand, that while finitesize effects are certainly present in our experiments, we believe that they do not dominate our measured torques. Before presenting these arguments, we would like to preface the discussion with a summary of past studies that have examined the role of finitesize effects on angular momentum transport in rotating shear flows. The work of Lesur & Longaretti (2005) used numerical simulations of rotating planeCouette flow up to Re ~ 10^{4} in the shearingsheet limit to conclude that Keplerianlike flows in TaylorCouette systems are strongly affected by Ekman circulation. The aforementioned experiments by the Princeton group (Ji et al. 2006) experimentally observed that angular momentum transport in their apparatus was only significant when they did not actively minimize Ekman circulation by varying the rotation rate of their axial end rings.
To further address this issue from a numerical standpoint, Avila (2012) performed direct numerical simulations of our experimental geometry as well as the Princeton apparatus (Ji et al. 2006; Schartman et al. 2009; Burin et al. 2010; Schartman et al. 2012). Avila found that the axial boundaries drive secondary flows that enhance the global angular momentum transport. The measured torques in those simulations were equal to the laminar value near Re = 0 and increased (approximately linearly) to be twice the laminar value in both the Maryland and Princeton geometry near his maximum Re ≈ 5000. While it was clear that finitesize effects played a dominant role for Re < 5000, Avila concluded by stating that the universal scaling of the torque with Reynolds number observed by Paoletti & Lathrop (2011) indicates that shear mechanisms might overwhelm finitesize effects at the values of Re explored here.
The role of finitesize effects at the values of Re that we have explored remains an open question. In order to quantitatively determine their effects at Re ~ 10^{6} a series of future studies will be required, as discussed at the end of this section. We now turn to our arguments as to why finitesize effects may not dominate the flows that we have examined, with the caveat that we cannot rule out the possibility that secondary flows produced by endwall effects are one of the different mechanisms that may perturb our quasiKeplerian flows into a turbulent state (see e.g. Mukhopadhyay et al. 2005; Mukhopadhyay & Saha 2011, and references therein).
The normalized torque G/G_{0} is approximately constant for each value of R_{Ω} characterized by the present experiments. This indicates that the amplitude of the torque varies with R_{Ω}, however the scaling with Re is unchanged (see Fig. 5). Paoletti & Lathrop (2011) observed that their torque scaling for Rayleighstable and unstable flows agreed with the Prandtlvon Kármán description of Lathrop et al. (1992a); Lewis & Swinney (1999). The Twente data, initially presented by van Gils et al. (2011b), was welldescribed by the theoretical predictions of Eckhardt et al. (2007b) for all rotation numbers explored. If Ekman circulation significantly contributed to the torque for Rayleighstable flows, as argued by Schartman et al. (2012), then one would expect systematic disparities between these theoretical descriptions and the measured torques. As shown in Fig. 5, though, the torque scaling agrees well with the observations of Lewis & Swinney (1999) for the case Ω_{2} = 0 for all values of R_{Ω}. Avila (2012) also argued that this universal scaling with Re indicates that shear turbulence dominates at the Reynolds numbers that we have explored, although this does not prove that secondary flows did not have a role in initiating the shear turbulence.
The torques in the Maryland and Twente experiments are measured over only 56% of the axial length of the flow centered at the midheight of the apparatus. This design has been intentionally implemented such that the torque measurements are unaffected by flows within 2.58 radial gap widths of either axial boundary where Ekman circulation is strongest. Wendt’s experiments (Wendt 1933) had a free upper surface, which is therefore devoid of Ekman circulation. Even though Taylor’s measurements (Taylor 1936) were affected by Ekman circulation for Γ > 100, his measurements of the torque for Rayleighstable flows that are expected to be most affected by Ekman circulation agree with our measurements of counterrotating flows for the same value of R_{Ω}, where Ekman circulation is dwarfed by the dominant shear.
One of course wonders on whether this Ekman circulation caused by the corotating upper and lower plates affect the flow patterns. For laminar flow e.g. for purely outer cylinder rotation this clearly is the case (Coles & van Atta 1966; Hollerbach & Fournier 2004). However, we argue that the strong turbulence destroys such an axial dependence of the flow field. To check this assumption, we have measured the full turbulent velocity profile with laser doppler anemometry (LDA; van Gils et al. 2012). The result is shown in Fig. 7. Evidently, over the length of the central section of the inner cylinder where we measure the torque there is no visible zdependence of the mean velocity; the plate boundary layers only produce an axial dependence far above the domain of the central section of the inner cylinder.
Fig. 7 Finitesize effects may be characterized by axial profiles of the angular velocity Ω measured at the midgap (r = (a + b)/2) in the Twente experiment. In this example, the cylinder Reynolds numbers are Re_{1} = 1.0 × 10^{6} and Re_{2} = 0 (outer cylinder stationary). The global torque measurements are taken for 0.22 < z/L < 0.78 with the top boundary of these measurements indicated by the dashed line at z/L = 0.78. The resolution of the laserdoppler anemometry prohibits measurements of the angular velocity in the boundary layer near z/L = 1 where Ω = Ω_{2} = 0, in this case. 
The Princeton experiments (Ji et al. 2006; Schartman et al. 2009; Burin et al. 2010; Schartman et al. 2012) measure local velocity correlations to determine the global angular momentum flux, whereas the Maryland and Twente experiments directly measure the global angular momentum flux using precision calibrated forcearm measurements. The distinction between the measured quantities has made direct comparisons of the experiments difficult. To bridge this gap, Burin et al. (2010) recently used their local velocity measurements to determine the corresponding torque G. To compare to previous studies with Ω_{2} = 0 (Lathrop et al. 1992b,a; Lewis & Swinney 1999) Burin et al. (2010) fit the scaling of to log _{10}(Re ∗ c_{f}), where c_{f} ≡ G/Re^{2}, and determined a slope of 1.40 ± 0.16. The authors claim that this value agrees with the measured value of 1.52 reported by Lathrop et al. (1992b,a) and 1.56 measured in Lewis & Swinney (1999). However, the appropriate Prandtlvon Kármán scaling predicts the following relationship (Lathrop et al. 1992b,a; Lewis & Swinney 1999) (15)in contrast to the scaling shown in Fig. 5 of Burin et al. (2010). Furthermore, the fit parameters N and M are predicted to depend upon the radius ratio in the following way where κ = 0.40 is the von Kármán constant and . The radius ratio η = 0.35 in the Princeton experiments, therefore the Prandtlvon Kármán skin friction law predicts N = 5.76 and M = −3.15. These values do not agree with our analysis of the data in Burin et al. (2010) where N ≈ 2 and M ≈ −0.4. In fact, the measured values of G determined by the local velocity fluctuations are on average five times larger than those predicted by the Prandtlvon Kármán skin friction law that has been verified using direct torque measurements (Lathrop et al. 1992b,a; Lewis & Swinney 1999; Paoletti & Lathrop 2011). Therefore, we argue that the local velocity fluctuation measurements used in the Princeton experiments (Ji et al. 2006; Schartman et al. 2009; Burin et al. 2010; Schartman et al. 2012) face severe experimental challenges. In fact, Huisman et al. (2012) showed that the local angular momentum transport undergoes fluctuations that are two orders of magnitude larger than the mean value. However, once the local angular momentum transport is averaged long enough and over a large enough region, Huisman et al. (2012) achieved perfect agreement between the local and the global measurements.
Clearly the contrasting conclusions of the Princeton experiments (Ji et al. 2006; Schartman et al. 2009; Burin et al. 2010; Schartman et al. 2012) and those presented here warrant further experimental and theoretical investigation, as suggested by Balbus (2011). In particular the role of finitesize effects must be better understood at Re ~ 10^{6}. It may be that the Princeton measurements of the local velocity fluctuations may not accurately determine the global angular momentum transport (Burin et al. 2010), due to lack of convergence. On the other hand, the effects of the axial boundaries on the global torque measurements presented here have not yet been characterized in detail. The Twente experiments (Huisman et al. 2012) provide both local velocities as well as the global torque, which thereby presents future opportunities to clarify these distinctions. Vice versa, direct global torque measurements in a split axialring apparatus, such as the Princeton device, would also be scientifically useful. New experiments that also measure the angular momentum transport as a function of aspect ratio would also be very interesting.
An explanation for the contrasting results of our measurements with those of past studies can be sought in both future experiments and numerical simulations. From an experimental point of view, an apparatus that is capable of simultaneously measuring the global angular momentum transport and controlling secondary circulation by independently varying the rotation rate of split axialrings would be particularly fruitful. In essence, such an apparatus would combine the techniques utilized in the Twente and Maryland experiments with the apparatus of the Princeton group (Ji et al. 2006; Schartman et al. 2009; Burin et al. 2010; Schartman et al. 2012). This would remove the ambiguities that are present in interpreting data from these experiments.
Avila (2012) observed that the torque increased (approximately) linearly with Re and was no more than twice the laminar value for Re < 5000. However, our measured torques are typically two orders of magnitude greater than the laminar value and increase faster than G ∝ Re, thus indicating a transition. Additional experiments could aid future numerical studies by performing measurements at lower Reynolds number to determine when the transition to turbulence occurs. In this way, computational studies could focus their efforts on examining values of the Reynolds number that straddle the transition point. Furthermore, experimentally characterizing the angular momentum transport below the transition will also be important in determining the torque produced by secondary flows.
In addition to overcoming these experimental challenges, efforts must be made to design laboratory systems that more closely resemble the astrophysical flows of interest. In accretion disks the radial and axial length scales are comparable (Regev & Umurhan 2008). However, many laboratory experiments (see Table 1) are designed with large aspect ratios to minimize finitesize effects. While the results in Fig. 4 seem to capture some of the dependence on the radius ratio, systematic studies with varying η are still required to determine the precise scaling. It also remains to be seen if our results are broadly applicable to smaller aspect ratios. The radial boundaries present in laboratory experiments produce boundary layers that affect the global angular momentum transport (Eckhardt et al. 2007b). Such boundaries may be less important in accretion flows and therefore one must account for these effects when extrapolating to astrophysicallyrelevant control parameters. Furthermore, recent numerical simulations by Meheut et al. (2010) have indicated that stratification may also play an important role in the dynamics of accretion disks, but such effects have not been experimentally examined in high Reynolds number Taylor Couette flow. Although these flows do not capture the full complexity of astrophysical systems, they do serve as an indication that hydrodynamic instabilities can occur in Rayleighstable flows. The detailed mechanism that produces the instability remains an open question for future endeavor.
5. Conclusions
The measurements that we present here indicate that the dimensionless torque G may be described as a product of functions that separately depend upon the Reynolds number Re and the rotation number R_{Ω}. The rotation number R_{Ω} introduced by Dubrulle et al. (2005) collapses all of the experimental data presented here for various radius ratios, aspect ratios and Reynolds numbers (see Table 1). The effects of global rotation, measured by G/G_{0}, where G_{0} ≡ G(Re,R_{Ω} = 0), are shown to be welldescribed by the function f(R_{Ω}) given in Eq. (12) for the entire range of R_{Ω} explored in the present studies.
The most astrophysically relevant result is the scaling of G/Re^{2}, which is proportional to both the turbulent viscosity parameter β and the accretion rate Ṁ. We observe that the expected accretion rate for quasiKeplerian flows (R_{Ω} ≤ −1) is approximately 14% of the maximum attainable rate for a given Reynolds number. We therefore get a dimensionless angular transport parameter β_{Md} = 2 × 10^{5}, in agreement with Richard and Zahn but more than an order of magnitude larger than the Princeton experiments. Such angular momentum transport is able to produce dimensionless accretion rates on the order of , which are compatible with observations in disks around T Tauri stars (Hersant et al. 2005). We have argued that our results are not easily attributed to finitesize effects, such as Ekman circulation. As such, we conclude that hydrodynamics may be able to transport angular momentum at astrophysical rates in spite of the linear stability provided by the radiallyincreasing angular momentum profile. This level of transport must result from turbulent means, thereby implying that quasiKeplerian flows can be nonlinearly unstable to finite amplitude disturbances.
Acknowledgments
The Maryland group would like to thank B. Eckhardt, Michael E. Fisher, C. Kalelkar, D. Martin, Harry L. Swinney and D. S. Zimmerman and acknowledge the support of Grant No. NSFDMR 0906109. B.D. thanks the CNRS for its continuous unconditional financial support that made this fundamental research possible. The Twente collaboration thanks G. W. Bruggert for crucial work in building the T^{3}C device, S. Grossmann and S. G. Huisman for discussions, and STW, which is financially supported by NWO, for financial support of this project.
References
 Abramowicz, M., Brandenburg, A., & Lasota, J.P. 1996, MNRAS, 281, L21 [NASA ADS] [CrossRef] [Google Scholar]
 Avila, M. 2012, Phys. Rev. Lett., 108, 124501 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Balbus, S. A. 2011, Nature, 470, 475 [NASA ADS] [CrossRef] [Google Scholar]
 Balbus, S. A., Hawley, J. F., & Stone, J. M. 1996, ApJ, 467, 76 [NASA ADS] [CrossRef] [Google Scholar]
 Beckwith, K., Armitage, P. J., & Simon, J. B. 2011, MNRAS, 416, 361 [NASA ADS] [Google Scholar]
 Brandenburg, A., Nordlund, A., Stein, R. F., & Torkelsson, U. 1995, ApJ, 446, 741 [NASA ADS] [CrossRef] [Google Scholar]
 Burin, M. J., Schartman, E., & Ji, H. 2010, Exp. Fluids, 48, 763 [CrossRef] [Google Scholar]
 Canuto, V. M., Goldman, I., & Hubickyj, O. 1984, ApJ, 280, L55 [NASA ADS] [CrossRef] [Google Scholar]
 Coles, D., & van Atta, C. 1966, J. Fluid Mech., 25, 513 [NASA ADS] [CrossRef] [Google Scholar]
 Drecker, A., Hollerbach, R., & Rudiger, G. 1998, MNRAS, 298, 1030 [NASA ADS] [CrossRef] [Google Scholar]
 Dubrulle, B. 1992, A&A, 266, 592 [NASA ADS] [Google Scholar]
 Dubrulle, B., & Hersant, F. 2002, EPJ B, 26, 379 [NASA ADS] [Google Scholar]
 Dubrulle, B., Dauchot, O., Daviaud, F., et al. 2005, Phys. Fluids, 17, 095103 [Google Scholar]
 Eckhardt, B., Grossmann, S., & Lohse, D. 2007a, Europhys. Lett., 78, 24001 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Eckhardt, B., Grossmann, S., & Lohse, D. 2007b, J. Fluid Mech., 581, 221 [NASA ADS] [CrossRef] [Google Scholar]
 Esser, A., & Grossmann, S. 1996, Phys. Fluids, 8, 1814 [NASA ADS] [CrossRef] [Google Scholar]
 Fromang, S., & Papaloizou, J. 2007, A&A, 476, 1113 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Grossmann, S., & Lohse, D. 2011, Phys. Fluids, 23, 045108 [NASA ADS] [CrossRef] [Google Scholar]
 Hawley, J. F., Balbus, S. A., & Winters, W. F. 1999, ApJ, 518, 394 [NASA ADS] [CrossRef] [Google Scholar]
 Hersant, F., Dubrulle, B., & Huré, J.M. 2005, A&A, 429, 531 [Google Scholar]
 Hollerbach, R., & Fournier, A. 2004, in MHD Couette Flows: Experiments and Models, eds. R. Rosner, G. Rüdiger, & A. Bonanno, AIP Conf. Ser., 733, 114 [Google Scholar]
 Huisman, S. G., van Gils, D. P. M., Grossmann, S., Sun, C., & Lohse, D. 2012, Phys. Rev. Lett., 108, 024501 [NASA ADS] [CrossRef] [Google Scholar]
 Ji, H., Burin, M., Schartman, E., & Goodman, J. 2006, Nature, 444, 343 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 King, A. R., Pringle, J. E., & Livio, M. 2007, MNRAS, 376, 1740 [NASA ADS] [CrossRef] [Google Scholar]
 Lathrop, D. P., Fineberg, J., & Swinney, H. L. 1992a, Phys. Rev. A, 46, 6390 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Lathrop, D. P., Fineberg, J., & Swinney, H. L. 1992b, Phys. Rev. Lett., 68, 1515 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Lesur, G., & Longaretti, P.Y. 2005, A&A, 444, 25 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Lewis, G. S., & Swinney, H. L. 1999, Phys. Rev. E, 59, 5457 [NASA ADS] [CrossRef] [Google Scholar]
 Meheut, H., Casse, F., Varniere, P., & Tagger, M. 2010, A&A, 516, A31 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Mukhopadhyay, B. 2008, Int. J. Mod. Phys. D, 17, 467 [NASA ADS] [CrossRef] [Google Scholar]
 Mukhopadhyay, B., & Saha, K. 2011, Res. Astron. Astrophys., 11, 163 [NASA ADS] [CrossRef] [Google Scholar]
 Mukhopadhyay, B., Afshordi, N., & Narayan, R. 2005, ApJ, 629, 383 [NASA ADS] [CrossRef] [Google Scholar]
 Paoletti, M. S., & Lathrop, D. P. 2011, Phys. Rev. Lett., 106, 024501 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Pringle, J. E. 1981, ARA&A, 19, 137 [NASA ADS] [CrossRef] [Google Scholar]
 Pumir, A. 1996, Phys. Fluids, 8, 3112 [NASA ADS] [CrossRef] [Google Scholar]
 Regev, O., & Umurhan, O. M. 2008, A&A, 481, 21 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Richard, D. 2001, Ph.D. Thesis, Univ. Paris VII [Google Scholar]
 Richard, D., & Zahn, J. 1999, A&A, 347, 734 [NASA ADS] [Google Scholar]
 Rozyczka, M., & Spruit, H. C. 1993, ApJ, 417, 677 [NASA ADS] [CrossRef] [Google Scholar]
 Schartman, E., Ji, H., & Burin, M. J. 2009, Rev. Sci. Instrum., 80, 024501 [NASA ADS] [CrossRef] [Google Scholar]
 Schartman, E., Ji, H., Burin, M. J., & Goodman, J. 2012, A&A, 543, A94 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Shakura, N. I., & Sunyaev, R. A. 1973, A&A, 24, 337 [NASA ADS] [Google Scholar]
 Stone, J. M., Hawley, J. F., Gammie, C. F., & Balbus, S. A. 1996, ApJ, 463, 656 [NASA ADS] [CrossRef] [Google Scholar]
 Taylor, G. I. 1936, Roy. Soc. London Proc. A, 157, 546 [Google Scholar]
 Umurhan, O. M., & Regev, O. 2004, A&A, 427, 855 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 van den Berg, T. H., Doering, C. R., Lohse, D., & Lathrop, D. P. 2003, Phys. Rev. E, 68, 036307 [NASA ADS] [CrossRef] [Google Scholar]
 van den Berg, T. H., Luther, S., Lathrop, D. P., & Lohse, D. 2005, Phys. Rev. Lett., 94, 044501 [NASA ADS] [CrossRef] [Google Scholar]
 van den Berg, T. H., van Gils, D. P. M., Lathrop, D. P., & Lohse, D. 2007, Phys. Rev. Lett., 98, 084501 [NASA ADS] [CrossRef] [Google Scholar]
 van Gils, D. P. M., Bruggert, G.W., Lathrop, D. P., Sun, C., & Lohse, D. 2011a, Rev. Scientific Instrum., 82, 025105 [NASA ADS] [CrossRef] [Google Scholar]
 van Gils, D. P. M., Huisman, S. G., Bruggert, G.W., Sun, C., & Lohse, D. 2011b, Phys. Rev. Lett., 106, 024502 [NASA ADS] [CrossRef] [Google Scholar]
 van Gils, D. P. M., Huisman, S. G., Grossmann, S., Sun, C., & Lohse, D. 2012, J. Fluid Mech., 706, 118149 [CrossRef] [Google Scholar]
 Wendt, F. 1933, Ing. Arch., 4, 577 [Google Scholar]
 Zeldovich, Y. B. 1981, Roy. Soc. London Proc. A, 374, 299 [NASA ADS] [CrossRef] [Google Scholar]
All Tables
TaylorCouette control parameters related to some astrophysical disks, as computed by Hersant et al. (2005).
All Figures
Fig. 1 TaylorCouette flow may be used to study angular momentum transport in rotating shear flows. The fluid is sheared between two independently rotating cylinders of radii a < b that rotate at angular velocities Ω_{1} and Ω_{2} for the inner and outer cylinders, respectively. Although the total fluid height is given by L, some experiments only measure the contribution to the torque over a central section of length L_{mid} to minimize end effects, as in (Lathrop et al. 1992b,a; Lewis & Swinney 1999; van den Berg et al. 2003, 2005, 2007; Paoletti & Lathrop 2011; van Gils et al. 2011b). 

In the text 
Fig. 2 a) Our experiments span a large range of the Reynolds number Re, which controls the turbulence intensity, and the rotation number R_{Ω}, introduced by Dubrulle et al. (2005), which compares shear to overall rotation. The rotation number can be used to distinguish between Rayleighstable flows (R_{Ω} ≤ −1 or R_{Ω} ≥ (1 − η)/η) and those that are linearly unstable (−1 < R_{Ω} < (1 − η)/η). b) All of our measurements for −1 < R_{Ω} < 0.38 are well above the linear stability curve (blue line) described by Esser & Grossmann (1996) and given by Eq. (8). The data are taken from separate experiments by van Gils et al. (2011b) (red squares) and (Paoletti & Lathrop 2011) (black circles). 

In the text 
Fig. 3 The scaling of the dimensionless torque G with the Reynolds number Re is independent of the rotation number R_{Ω}, however the amplitude varies as in Paoletti & Lathrop (2011); van Gils et al. (2011b). The measurements by Paoletti & Lathrop (2011) are in black circles while the data from van Gils et al. (2011b) are shown by red squares. The thick blue line indicates the theoretical value for purely laminar flow, where angular momentum is transported only by molecular viscosity. 

In the text 
Fig. 4 a) The dimensionless torque G normalized by G_{0} ≡ G(Re,R_{Ω} = 0) for different values of the radius ratio η nicely collapses when plotted as function of R_{Ω}. The data from Wendt (1933) are shown as cyan (η = 0.68), blue (η = 0.85) and green (η = 0.935) triangles. Additional radius ratios are examined using the data from Taylor (1936), shown as orange diamonds, Richard (Richard 2001; Dubrulle et al. 2005), given by magenta squares, Paoletti & Lathrop (2011) indicated by black circles and van Gils et al. (2011b) by red circles. The solid lines are fits given by Eq. (12). Keplerian flow states are indicated by the dashed line at R_{Ω} = −4/3. In b) we focus on the peak of the curve shown in a), but only present the data from Twente (van Gils et al. 2011b) (red) and Maryland (Paoletti & Lathrop 2011) (black). The solid line is the fit (12). 

In the text 
Fig. 5 The dimensionless torque G may be compensated by the fit f(R_{Ω}) given by Eq. (12). The data from both Paoletti & Lathrop (2011) (black circles) and van Gils et al. (2011b) (red squares) agree with the best fit from Lewis & Swinney (1999) for the case where the outer cylinder was stationary (blue line). 

In the text 
Fig. 6 The scaling of a) G/Re^{2}, which is proportional to the accretion rate Ṁ and viscosity parameter β, decays slowly with Re while having an amplitude that varies with the rotation number R_{Ω} (see Fig. 4). b) The effects of global rotation can be accounted for by compensating G/Re^{2} by the fits f(R_{Ω}) given in Eq. (12). The measurements from Twente are shown as red squares. The Maryland data are given by black circles, except for quasiKeplerian flows (R_{Ω} ≤ −1), which are indicated by blue diamonds. The green continuous line is the theoretical fit given in Eq. (14) normalized by f(R_{Ω} = −0.2755), which corresponds to Ω_{2} = 0. 

In the text 
Fig. 7 Finitesize effects may be characterized by axial profiles of the angular velocity Ω measured at the midgap (r = (a + b)/2) in the Twente experiment. In this example, the cylinder Reynolds numbers are Re_{1} = 1.0 × 10^{6} and Re_{2} = 0 (outer cylinder stationary). The global torque measurements are taken for 0.22 < z/L < 0.78 with the top boundary of these measurements indicated by the dashed line at z/L = 0.78. The resolution of the laserdoppler anemometry prohibits measurements of the angular velocity in the boundary layer near z/L = 1 where Ω = Ω_{2} = 0, in this case. 

In the text 
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.